{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2021:P2NGTLOJR6ZDQWPPRV5XX4GMLJ","short_pith_number":"pith:P2NGTLOJ","schema_version":"1.0","canonical_sha256":"7e9a69adc98fb23859ef8d7b7bf0cc5a774fa3e049b679738397309ad8197d12","source":{"kind":"arxiv","id":"2109.00191","version":2},"attestation_state":"computed","paper":{"title":"Realistic neutron star models in $f(T)$ gravity","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.HE"],"primary_cat":"gr-qc","authors_text":"Rui-Hui Lin, Xiang-Hua Zhai, Xiao-Ning Chen","submitted_at":"2021-09-01T05:21:03Z","abstract_excerpt":"We investigate the nonrotating neutron stars in $f(T)$ gravity with $f(T)=T+\\alpha{T}^2$, where $T$ is the torsion scalar in the teleparallel formalism of gravity. In particular, we utilize the SLy and BSk family of equations of state for perfect fluid to describe the neutron stellar matter and search for the effects of the $f(T)$ modification on the models of neutron stars. For positive $\\alpha$, the modification results in a smaller stellar mass in comparison to general relativity, while the neutron stars will contain larger amount of matter for negative $\\alpha$. Moreover, there seems to be"},"verification_status":{"content_addressed":true,"pith_receipt":true,"author_attested":false,"weak_author_claims":0,"strong_author_claims":0,"externally_anchored":false,"storage_verified":false,"citation_signatures":0,"replication_records":0,"graph_snapshot":true,"references_resolved":false,"formal_links_present":false},"canonical_record":{"source":{"id":"2109.00191","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"gr-qc","submitted_at":"2021-09-01T05:21:03Z","cross_cats_sorted":["astro-ph.HE"],"title_canon_sha256":"0426407ee940d85882145c1635d6ccd3b78a4dc632b813a580d7ae2807598f29","abstract_canon_sha256":"2cec36652b9e7be65bbac4e41485524c9af1a1884d3275d8748e39bb2a200613"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T04:18:01.517953Z","signature_b64":"fOEsRv9R30Mk/GlGWcpJHrS1VVd/I7xMmJUGuyGNoLfegpYSPMZfMyzfh6BylYLvOgosy3mo+3EyijV+PRcdAg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"7e9a69adc98fb23859ef8d7b7bf0cc5a774fa3e049b679738397309ad8197d12","last_reissued_at":"2026-07-05T04:18:01.517386Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T04:18:01.517386Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Realistic neutron star models in $f(T)$ gravity","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.HE"],"primary_cat":"gr-qc","authors_text":"Rui-Hui Lin, Xiang-Hua Zhai, Xiao-Ning Chen","submitted_at":"2021-09-01T05:21:03Z","abstract_excerpt":"We investigate the nonrotating neutron stars in $f(T)$ gravity with $f(T)=T+\\alpha{T}^2$, where $T$ is the torsion scalar in the teleparallel formalism of gravity. In particular, we utilize the SLy and BSk family of equations of state for perfect fluid to describe the neutron stellar matter and search for the effects of the $f(T)$ modification on the models of neutron stars. For positive $\\alpha$, the modification results in a smaller stellar mass in comparison to general relativity, while the neutron stars will contain larger amount of matter for negative $\\alpha$. Moreover, there seems to be"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2109.00191","kind":"arxiv","version":2},"verdict":{"id":null,"model_set":{},"created_at":null,"strongest_claim":"","one_line_summary":"","pipeline_version":null,"weakest_assumption":"","pith_extraction_headline":""},"integrity":{"clean":true,"summary":{"advisory":0,"critical":0,"by_detector":{},"informational":0},"endpoint":"/pith/2109.00191/integrity.json","findings":[],"available":true,"detectors_run":[],"snapshot_sha256":"c28c3603d3b5d939e8dc4c7e95fa8dfce3d595e45f758748cecf8e644a296938"},"references":{"count":0,"sample":[],"resolved_work":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57","internal_anchors":0},"formal_canon":{"evidence_count":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"author_claims":{"count":0,"strong_count":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"builder_version":"pith-number-builder-2026-05-17-v1"},"aliases":[{"alias_kind":"arxiv","alias_value":"2109.00191","created_at":"2026-07-05T04:18:01.517450+00:00"},{"alias_kind":"arxiv_version","alias_value":"2109.00191v2","created_at":"2026-07-05T04:18:01.517450+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2109.00191","created_at":"2026-07-05T04:18:01.517450+00:00"},{"alias_kind":"pith_short_12","alias_value":"P2NGTLOJR6ZD","created_at":"2026-07-05T04:18:01.517450+00:00"},{"alias_kind":"pith_short_16","alias_value":"P2NGTLOJR6ZDQWPP","created_at":"2026-07-05T04:18:01.517450+00:00"},{"alias_kind":"pith_short_8","alias_value":"P2NGTLOJ","created_at":"2026-07-05T04:18:01.517450+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":2,"internal_anchor_count":0,"sample":[{"citing_arxiv_id":"2605.30369","citing_title":"Reconciling GW170817 and GW190814 with a Nonmonotonic Sound-Speed Equation of State","ref_index":50,"is_internal_anchor":false},{"citing_arxiv_id":"2512.19207","citing_title":"Static plane symmetric solutions in $f(Q)$ gravity","ref_index":16,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/P2NGTLOJR6ZDQWPPRV5XX4GMLJ","json":"https://pith.science/pith/P2NGTLOJR6ZDQWPPRV5XX4GMLJ.json","graph_json":"https://pith.science/api/pith-number/P2NGTLOJR6ZDQWPPRV5XX4GMLJ/graph.json","events_json":"https://pith.science/api/pith-number/P2NGTLOJR6ZDQWPPRV5XX4GMLJ/events.json","paper":"https://pith.science/paper/P2NGTLOJ"},"agent_actions":{"view_html":"https://pith.science/pith/P2NGTLOJR6ZDQWPPRV5XX4GMLJ","download_json":"https://pith.science/pith/P2NGTLOJR6ZDQWPPRV5XX4GMLJ.json","view_paper":"https://pith.science/paper/P2NGTLOJ","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2109.00191&json=true","fetch_graph":"https://pith.science/api/pith-number/P2NGTLOJR6ZDQWPPRV5XX4GMLJ/graph.json","fetch_events":"https://pith.science/api/pith-number/P2NGTLOJR6ZDQWPPRV5XX4GMLJ/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/P2NGTLOJR6ZDQWPPRV5XX4GMLJ/action/timestamp_anchor","attest_storage":"https://pith.science/pith/P2NGTLOJR6ZDQWPPRV5XX4GMLJ/action/storage_attestation","attest_author":"https://pith.science/pith/P2NGTLOJR6ZDQWPPRV5XX4GMLJ/action/author_attestation","sign_citation":"https://pith.science/pith/P2NGTLOJR6ZDQWPPRV5XX4GMLJ/action/citation_signature","submit_replication":"https://pith.science/pith/P2NGTLOJR6ZDQWPPRV5XX4GMLJ/action/replication_record"}},"created_at":"2026-07-05T04:18:01.517450+00:00","updated_at":"2026-07-05T04:18:01.517450+00:00"}